The surface brightness profile is from Thomsen & Baum (1987) in 523nm. Here we
used our data for V < 26.5, slightly fainter than the normal completeness limit,
but we were forced to do this to obtain any kind of estimate of the radial
falloff of the GCS. Within the large uncertainties of the GC counts, there is no
difference between the GCS distribution and the halo light.
For V < 26.0 there are ~= 25 GCs after background subtraction and within
radii 3" < r < 30". To these we add about 25% more as an estimate of the number
of GCs lying in the innermost and outermost regions (r < 3", r > 30") not
covered by our data. Then, to correct the total for the GCs fainter than our
adopted limit of V = 26, we note that this limit is 1.73 mag or 1.23 standard
deviations brighter than the mean GCLF turnover (previous section). This range
includes 11% of the true total cluster population. We therefore scale up the
observed number by a factor of 9. With M^t^_V_ = -21.46 (Table 1) we then obtain
S_N_ = 0.77 +/- 0.21, in very good agreement with the earlier estimate of S_N_ ~
1.0 by Baum et al. (1995). This strikingly low-S_N_ value is at the bottom end
of the observed range for any type of E galaxy, regardless of luminosity or
environment. Our value may in fact even be a slight overestimate if the galaxy
actually has no clusters beyond the 30" (15 kpc) radius.
In the Coma Cluster
A.J., 71, 635, 1966.
A.J., 73, 442, 1968.
A.J., 77, 642, 1972.
Ap. J., 158, 657, 1969.
A.J., 79, 671, 1974.
E1 (de Vaucouleurs)
RA = 12 57 33, DEC = 28 31.0 (CGCG)
18' north center of Coma I cluster
(B-V)(0) is interpolated.